Motions in the interiors and atmospheres of Jupiter and Saturn. II - Barotropic instabilities and normal modes of an adiabatic planet

Details Motions in the interiors and atmospheres of Jupiter and Saturn. II - Barotropic instabilities and normal modes of an adiabatic planet Motions in the interiors and atmospheres of Jupiter and Saturn. II - Barotropic instabilities and normal modes of an adiabatic planet

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icar...65..370i&link_type=abstract

Icarus (ISSN 0019-1035), vol. 65, Feb.-Mar. 1986, p. 370-382. NASA-supported research.

Mathematics

14

Atmospheric Circulation, Jupiter Atmosphere, Planetary Cores, Saturn Atmosphere, Barotropism, Galerkin Method, Mathematical Models, Oscillations, Rossby Regimes, Wave Propagation, Planets, Jupiter, Giant Planets, Saturn, Motion, Barotropy, Dynamics, Atmosphere, Interior, Amplitude, Density, Surface, Perturbations, Oscillations, Structure, Velocity, Wavelengths, Analysis, Flow

Scientific paper

A rotating and adiabatic inviscid fluid planet possesses low frequency motions that are barotropic, quasi-geostrophic and quasi-columnar. The limiting curvature at which flow becomes unstable upon projection onto the planetary surface is negative, with an amplitude that is 3-4 times that for thin atmospheres, in planets in which density linearly decreases to zero at the surface. This result is shown to hold for all quasi-columnar perturbations. Both the phase speed of the normal mode oscillations and the barotropic stability criterion have features in common with Saturn and Jupiter oscillations.

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